Abstract

We use multispacecraft observations to examine the spatial and temporal
distributions of energetic particles accelerated by shock waves driven
by coronal mass ejections from the Sun. The behavior of the intensity
time profiles ahead of the shock can depend strongly on the longitude of
the point where the observer's magnetic flux tube connects to the shock,
relative to the nose of the shock where acceleration is strongest.
Particle intensities can increase (decrease) with time as this point
swings eastward through >= 50° toward (away from) the shock nose
because of solar rotation. Well behind the shock, intensities are often
constant with longitude and the intensities of these quasi-trapped
particles at all energies decrease continuously with time over many days
as their containment volume expands. Delayed proton events are produced
when shocks expand into slow solar wind so they suddenly encounter an
observer's field line far from the Sun. Sunward flows are seen when the
shock passes over the observer or when it suddenly strikes his field
line at radial distances out beyond him.

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